Table 2.
Properties of Haro 11.
| Property | Unit | Value | Reference |
|---|---|---|---|
| Other name | ... | ESO 350-IG38 | 1 |
| RA (J2000) | h:m:s | 00:36:52.7 | 1 |
| Dec (J2000) | d:m:s | –33:33:17 | 1 |
| Vsys(optical) | km s−1 | 6194 ± 5.1 | 2 |
| Redshift | ... | 0.0206467 | 2 |
| Distance | Mpc | 87.2 ± 6.1 | 3 |
| Scale | pc/arcsec−1 | ∼420 | 3 |
| M* | 109 M⊙ | 2.6 ± 0.8 | 4 |
| Vsys (CO) | km s−1 | 6051.3 ± 2.1 | 4 |
| CO(1–0) flux | Jy km s−1 | 3.3 ± 0.1 | 4 |
| [C I] flux | Jy km s−1 | 7.4 ± 0.3 | 4 |
| MH2(CO) | 109 M⊙ | 3.8 |
4 |
| MH2([CI]) | 108 M⊙ | 2.1-5.3 | 4 |
| MHI | 108 M⊙ | 5.1 | 5 |
| SFRHα+TIR | M⊙ yr−1 |  |
6 |
| SFRHα(HST) | M⊙ yr−1 | 24.0 | 7 |
| SFRTIR | M⊙ yr−1 | 28.6 | 8 |
| SFRHα | M⊙ yr−1 | 25.1 ± 0.4 | 4 |
| Size | kpc2 | 12.5 | 4 |
| σv | km s−1 | 17.2 |
4 |
| Pturb | 106 K cm−3 | 3.4 |
4 |
| αvir | ... | 0.17 |
4 |
Notes. The Kroupa (2001) IMF is used to derive the stellar mass and SFR in this work. We assume the CO-H2 conversion factor αCO as 60 M⊙ (K km s−1 pc−2)−1, with a range of 10−110 M⊙ (K km s−1 pc−2)−1. We used the Python packages Statmorph to estimate the radius R80 containing 80% flux in r band, and then calculated the size of Haro 11. The CO(1–0) velocity dispersion σv, internal turbulent pressure Pturb and the viral parameter αvir are shown as the median values with one-sigma ranges. We also used the [C I] luminosity to derive the molecular gas based on the calibration in Madden et al. (2020) at metallicities of 0.25 Z⊙ and 0.1 Z⊙, respectively, with a systemic uncertainty of 0.3 dex.
References. (1) Östlin et al. (2015); (2) Menacho et al. (2021); (3) NED; (4) this work; (5) Pardy et al. (2016); (6) Rémy-Ruyer et al. (2015); (7) Hayes et al. (2007); (8) Madden et al. (2013).
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